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Cosmic ray and solar energetic particle flux in paleomagnetospheres

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Figure

Fig. 1. Geometry of the model magnetosphere.
Table 1. First column: Proton kinetic energies used in this study. Second column: Associated rigidity values
Fig. 3. Magnetospheric field lines of the magnetic field of zonal dipole inthe x-z plane (GSE coordinates)
Fig. 4.(a) Magnetospheric field lines of the magnetic field of a zonaldipole, (b) particle impact regions on the Earth (proton energy 4 GeV,g01 = 30000 nT), (c) cutoff latitudes and (d) impact area
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